Discovery of X-ray bursts from MXB 1728-34

Hoffman, Jeffrey A.; Lewin, W. H. G.; Doty, J.; Hearn, D. R.; Clark, G. W.; Jernigan, G.; Li, F. K.

doi:10.1086/182292

Cited by 50 publications

(28 citation statements)

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“…References. 1) Stella et al (1987); 2) Kuulkers et al (2003) White & Swank (1982); 38) Walter et al (1982); 39) Galloway et al (2008); 40) Becker et al (1977); 41) Lewin et al (1977); 42) Krimm et al (2007); 43) Altamirano et al (2010); 44) Ortolani et al (1994); 45) Galloway et al (2010); 46) Wilson-Hodge et al (2012); 47) Lewin et al (1976); 48) Hoffman et al (1976); 49) Strohmayer et al (1996); 50) Deutsch et al (2000); 51) in't Zand et al (1998); 52) Shahbaz et al (2008); 53) Hakala et al (2011); 54) Zhang et al (2012); 55) Kuulkers et al (2010); 56) Madej et al (2010); 57) Swank et al (1978); 58) Brandt et al (1992); 59) Ford et al (1997) Galactic plane. Table 1 presents an updated version of the UCXB and UCXB candidate overviews in in't Zand et al (2007), Lasota et al (2008) and Nelemans & Jonker (2010).…”

Section: Methodsunclassified

Long-term luminosity behavior of 14 ultracompact X-ray binaries

Haaften

Voss

Nelemans

2012

A&A

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Context. X-ray binaries are usually divided in persistent and transient sources. For ultracompact X-ray binaries (UCXBs), the mass transfer rate is expected to be a strong function of orbital period, predicting persistent sources at short periods and transients at long periods. Aims. For 14 UCXBs including two candidates, we investigate the long-term variability and average bolometric luminosity with the purpose of learning how often a source can be expected to be visible above a given luminosity, and we compare the derived luminosities with the theoretical predictions. Methods. We use data from the RXTE All-Sky Monitor because of its long-term, unbiased observations. Many UCXBs are faint, i.e., they have a count rate at the noise level for most of the time. Still, information can be extracted from the data, either by using only reliable data points or by combining the bright-end variability behavior with the time-averaged luminosity.Results. Luminosity probability distributions show the fraction of time that a source emits above a given luminosity. All UCXBs show significant variability and relatively similar behavior, though the time-averaged luminosity implies higher variability in systems with an orbital period longer than 40 min. Conclusions. There is no large difference in the statistical luminosity behavior of what we usually call persistent and transient sources. UCXBs with an orbital period below ∼30 min have a time-averaged bolometric luminosity that is in reasonable agreement with estimates based on the theoretical mass transfer rate. Around 40 min the lower bound on the time-averaged luminosity is similar to the luminosity based on the theoretical mass transfer rate, suggesting these sources are indeed faint when not detected. Above 50 min some systems are much brighter than the theoretical mass transfer rate predicts, unless these systems have helium burning donors or lose additional angular momentum.

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Section: Methodsunclassified

Long-term luminosity behavior of 14 ultracompact X-ray binaries

Haaften

Voss

Nelemans

2012

A&A

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“…The burst spectrum can be fitted by a blackbody with temperature increasing from 1 to 3 keV during the burst rise time. Most of these bursts show evidence for photospheric radius expansion (Hoffman et al 1976;White et al 1986;Day & Tawara 1900;Foster et al 1986;Franco 2001;van Straaten 2001;Galloway et al 2003Galloway et al , 2006. Flux oscillations at 363 Hz during the bursts were discovered in this source with the Rossi X-ray Timing Explorer (RXTE), and interpreted as the spin frequency of the NS (Strohmayer et al 1996;Chakrabarty et al 2003).…”

Section: The Source 4u 1728-34mentioning

confidence: 99%

The X-ray spectrum of the bursting atoll source 4U 1728-34 observed with INTEGRAL

Falanga

Götz²,

Goldoni

et al. 2006

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We present for the first time a study of the 3-200 keV broad band spectra of the bursting atoll source 4U 1728-34 (GX 354-0) along its hardness intensity diagram. The analysis was done using the INTEGRAL public and Galactic Center deep exposure data ranging from February 2003 to October 2004. The spectra are well described by a thermal Comptonization model with an electron temperature from 35 keV to 3 keV and Thomson optical depth, τ T , from 0.5 to 5 in a slab geometry. The source undergoes a transition from an intermediate/hard to a soft state where the source luminosity increases from 2 to 12% of Eddington. We have also detected 36 type I X-ray bursts two of which show photospheric radius expansion. The energetic bursts with photospheric radius expansion occurred at an inferred low mass accretion rate per unit area ofṁ ∼ 1.7 × 10 3 g cm −2 s −1 , while the others at a higher one between 2.4 × 10 3 −9.4 × 10 3 g m −2 s −1 . For 4U 1728-34 the bursts' total fluence, and the bursts' peak flux are anti-correlated with the mass accretion rate. The type I X-ray bursts involve pure helium burning either during the hard state, or during the soft state of the source.

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“…The optical counterpart of this "galactic bulge" source has not been identified yet, owing to the high optical extinction toward the Galactic center. Discovered in 1976 with the Small Astronomy Satellite SAS-3 Hoffman et al 1976), this source belongs to the so-called atoll class (Hasinger & van der Klis 1989) and shows frequent type-I X-ray bursts (e.g., Basinska et al 1984) that are caused by thermonuclear flashes on the neutron star surface. Furthermore, double-peaked burst profiles have been observed (Hoffman et al 1976), which are explained as caused by photospheric radius expansion during the burst (Taam 1982).…”

Section: Introductionmentioning

confidence: 99%

“…Discovered in 1976 with the Small Astronomy Satellite SAS-3 Hoffman et al 1976), this source belongs to the so-called atoll class (Hasinger & van der Klis 1989) and shows frequent type-I X-ray bursts (e.g., Basinska et al 1984) that are caused by thermonuclear flashes on the neutron star surface. Furthermore, double-peaked burst profiles have been observed (Hoffman et al 1976), which are explained as caused by photospheric radius expansion during the burst (Taam 1982). These bursts have been used to constrain the distance to the source, between 4.1 and 5.1 kpc (Di Salvo et al 2000;Galloway et al 2003).…”

Section: Introductionmentioning

confidence: 99%

X-ray spectroscopy of MXB 1728–34 withXMM-Newton

Egron

Salvo

Burderi

et al. 2011

A&A

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We analyzed an XMM-Newton observation of the low-mass X-ray binary and atoll source MXB 1728-34. The source was in a lowluminosity state during the XMM-Newton observation, corresponding to a bolometric X-ray luminosity of 5 × 10 36 d 2 5.1 kpc erg s −1 . The 1-11 keV X-ray spectrum of the source, obtained combining data from all the five instruments on-board XMM-Newton, is well fitted by a Comptonized continuum. Evident residuals are present at 6−7 keV, which are ascribed to the presence of a broad iron emission line. This feature can be equally well fitted by a relativistically smeared line or by a self-consistent, relativistically smeared reflection model. Under the hypothesis that the iron line is produced by reflection from the inner accretion disk, we can infer important information on the physical parameters of the system, such as the inner disk radius, R in = 25−100 km, and the inclination of the system, 44• < i < 60• .

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Discovery of X-ray bursts from MXB 1728-34

Cited by 50 publications

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Long-term luminosity behavior of 14 ultracompact X-ray binaries

Long-term luminosity behavior of 14 ultracompact X-ray binaries

The X-ray spectrum of the bursting atoll source 4U 1728-34 observed with INTEGRAL

X-ray spectroscopy of MXB 1728–34 withXMM-Newton

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